1. B.V. Jackson H.-S. Yu, P.P. Hick, A. Buffington, M. Tokumaru
Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA
M. Tokumaru
Institute for Space-Earth Environmental Research (ISEE), Nagoya University, Nagoya , Japan
A. Gonzalez-Espararza, J. Mejia-Ambriz, O. Chang
SCIESMEX, Instituto de Geofisica, UNAM, Morelia, Mexico
D. Odstrcil
George Mason University, Fairfax, Virginia, and NASA-Goddard Spaceflight Center, USA
S. Hong, J. Kim
Korean Space Weather Center, National Radio Research Agency, 198-6, Jeju, South Korea
Where necessary I will add comments
B. Lee, J. Yi, J. Yun
SELab, 8, Nonhyeon-ro 150-gil, Gangnam-gu, Seoul, South Korea
M.M Bisi
RAL Space, Science & Technology Facilities Council, Rutherford Appleton Laboratory, Harwell Oxford, Didcot, Oxfordshire, OX11 0QX, England (UK)
Masayoshi

2. Today’s Predictive Analysis
Where necessary I will add comments
Masayoshi

3. IPS Heliospheric Analyses ISEE (STELab)
DATA
IPS Heliospheric Analyses ISEE (STELab)
The STELab interplanetary scintillation 327 MHz remote-sensing cylindrical parabola near Mt. Fuji is shown. The array moves in declination to provide views of sources at different locations in the sky as they pass overhead. The other array of this type is at Kiso, to the north of Toyokawa.
ISEE IPS array near Mt. Fuji
ISEE IPS array systems

4. IPS Heliospheric Analyses ISEE (STELab)
DATA
IPS Heliospheric Analyses ISEE (STELab)
Density inhomogenieties in the solar wind on the order of 150 km size from point radio sources produce an intensity pattern variation on the ground that travels away from the Sun with the solar wind speed. This pattern, measured and correlated between different radio sites in Japan allows a determination of the solar wind speed by translating this value to the line of sight perpendicular. The fuzz observed correlates from one radio site to another.
IPS line-of-sight response
ISEE IPS array systems

5. IPS line-of-sight response Sample outward motion over time
Jackson, B.V., et al., 2008, Adv. in Geosciences, 21,
Heliospheric C.A.T. analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction.
ISEE IPS
This shows how the UCSD IPS time-dependent Computer Assisted Tomography (C.A.T.) analysis works. The 327 MHz IPS line of sight weighting provides a weight for each source observation on a spherical source surface below each line. As material moves outward from the Sun, it follows a very specific modeled path and expansion that is weighted differently at different times. The full mathematical treatment can be found in Jackson, B.V., et al., 2008, Adv. in Geosciences, 21,
Sample outward motion over time

6. Space Weather Predictions using IPS
Heliospheric C.A.T. analyses: example line-of-sight distribution for each sky location to form the source surface of the 3D reconstruction.

7. CSSS model Source surface Br field component sample
(Zhao, X. P. and Hoeksema, J. T., 1995, J. Geophys. Res., 100 (A1), 19.)
CSSS model
Dunn et al., 2005, Solar Physics 227: 339–353.
Source surface Br field component sample
Inner region: the CSSS model calculates the magnetic field using photospheric measurements and a horizontal current model.
2. Middle region: the CSSS model opens the field lines. In the outer region.
3. Outer region: the UCSD tomography convects the magnetic field along velocity flow lines.

8. Today’s Real-Time SOLIS CSSS Open-Field Predictions
Today’s Real-Time SOLIS CSSS Open-Field Predictions
M Potentaily talk will proceed this way

9. Today’s Real-Time SOLIS CSSS Open-Field Correlations
Today’s Real-Time SOLIS CSSS Open-Field Correlations
M Potentaily talk will proceed this way

10. IPS Get-together at UCSD
 UCSD IPS Workshop December –
First Announcement
Bernard V. Jackson
J. Americo Gonzalez-Esparza
Mario M. Bisi
Munetoshi Tokumaru
Dear Colleagues,
We will be having a small IPS-based workshop (including associated Faraday rotation prospects) held December, 2016, in La Jolla, CA, USA, at UCSD immediately following the 2016 fall AGU meeting in San Francisco, CA, USA.
This mini-workshop was decided-upon as a good time to present updated results from the Third Remote Sensing Workshop held October, 2015 in Morelia, Michoacan, Mexico.

11. IPS Get-together at UCSD
Tentative agenda:
(1) Progress towards international WIPSS organization and collaborative efforts.
(2)  Single and multi-site IPS analyses and comparisons (including the determination of accurate velocity and g-level values with errors).
(a) Different methods of determining single-site speeds.
(b) Different methods of determining error values for IPS speeds and g-levels -
which techniques work best, and why.
(c) Different methods of IPS data presentation – skymaps, timeseries, etc.
(d) IPS tomographic data representations of these data sets.
(e) Use of these data sets with heliospheric 3D-MHD analyses. (3)  Progress toward providing the simplified ASCII (txt file) IPS output (IPSCDFv1.0), the agreed-upon standard data format, from all sites; its implementation in near real time, and as an archival data set.
(a) Best ways to provide IPS g-levels in near real time.
(b) Provision of more complete IPS data sets for colleague access at host sites.
(4)  Heliospheric Faraday rotation (FR) experiment design and implementation including discussion on progress thus far achieved and/or published.

12. ORIGINALD ANALYSIS (White Light)
Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi: /2008JA013224
27-28 May 2003 CME event period
ORIGINALD ANALYSIS (White Light)
Full SMEI data set, 6-hour cadence, 3º x 3º lat, long
SMEI proton density reconstruction for the May 2003 halo CME sequence. Reconstructed and ACE L2 in-situ densities are compared over one Carrington rotation.

13. SMEI Webpages - http://smei.ucsd.edu
The SMEI instrument was closed by the Air Force in September 2011, UCSD maintains the only SMEI Web pages and has upgraded them at: SMEI high resolution tomography has been used to reconstruct a filament at 1 AU!
SMEI Webpages -

14. Future? Cut-away and schematic Characteristics
Jackson,B.V., et al., 2004, Solar Phys., 225,
All sky view to within 2º (7.5Rs) of the Sun
SMEI heritage
Future?
Cut-away and schematic
Characteristics
Jackson,B.V., et al., 2010, Solar Phys., 265, 257–275.

15. Instrumentation Accomodation
Future?
PERSEUS
Instrumentation Accomodation